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The Euphrosyne Family's Contribution to the Low Albedo Near-Earth Asteroids

Masiero, Joseph R. and Carruba, V. and Mainzer, A. and Bauer, J. M. and Nugent, C. (2015) The Euphrosyne Family's Contribution to the Low Albedo Near-Earth Asteroids. Astrophysical Journal, 809 (2). Art. No. 179. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20151019-112709959

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Abstract

The Euphrosyne asteroid family is uniquely situated at high inclination in the outer Main Belt, bisected by the ν_6 secular resonance. This large, low albedo family may thus be an important contributor to specific subpopulations of the near-Earth objects. We present simulations of the orbital evolution of Euphrosyne family members from the time of breakup to the present day, focusing on those members that move into near-Earth orbits. We find that family members typically evolve into a specific region of orbital element-space, with semimajor axes near ~3 AU, high inclinations, very large eccentricities, and Tisserand parameters similar to Jupiter family comets. Filtering all known Near-Earth objects (NEOs) with our derived orbital element limits, we find that the population of candidate objects is significantly lower in albedo than the overall NEO population, although many of our candidates are also darker than the Euphrosyne family, and may have properties more similar to comet nuclei. Followup characterization of these candidates will enable us to compare them to known family properties, and confirm which ones originated with the breakup of (31) Euphrosyne.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/809/2/179 DOIArticle
http://iopscience.iop.org/article/10.1088/0004-637X/809/2/179/metaPublisherArticle
http://arxiv.org/abs/1507.07887arXivDiscussion Paper
ORCID:
AuthorORCID
Masiero, Joseph R.0000-0003-2638-720X
Additional Information:© 2015 American Astronomical Society. Received 2015 May 22; accepted 2015 July 17; published 2015 August 21. This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. J. M. was funded by a NASA Planetary Geology and Geophysics grant, and through the JPL internal Research and Technology Development program. V. C. was supported by the FAPESP grant 2014/06762-2. The authors would like to thank UNESP, CAPES, AAB, and FAPESP for supporting the 2014 Small Bodies Dynamics conference in Ubatuba, Brazil, which inspired this work. The JPL High-Performance Computing Facility used for our simulations is supported by the JPL Office of the CIO. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
JPL Internal Research and Technology Development ProgramUNSPECIFIED
Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)2014/06762-2
Subject Keywords:minor planets, asteroids: general
Issue or Number:2
Record Number:CaltechAUTHORS:20151019-112709959
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20151019-112709959
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:61258
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:19 Oct 2015 18:36
Last Modified:03 Oct 2019 09:05

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